The uncertainty in the above positions is stated to be +/- 0".2 in eachcoordinate. Additional approximate magnitudes for 2010jp, which is locatedin the field of the merging galaxy IC 2163: Oct. 16.32, [18.5; 22.23,[18.0; Nov. 12.14, 17.4. Additional approximate magnitudes for 2010jq:Apr. 15.08, [18.5; May 13.00, [18.5; Nov. 12.30, 17.1.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars.

T. Boles, Coddenham, England, reports the discovery of an apparentsupernova (mag 18.1) on unfiltered CCD images taken on Nov. 7.075 UT with a0.35-m reflector. The new object is located at R.A. = 8h16m49s.66, Decl. =+60o29'46".1 (equinox 2000.0), which is approximately 2".6 east and 11".2north of the center of UGC 4294. Boles also measured position end figures49s.63, 45".8 and magnitude V = 18.3 on Nov. 9.544 using an image (limitingmag 20.0) taken with the 0.61-m Cassegrain reflector at the Sierra StarsObservatory (Alpine County, California). Nothing is present at this positionon Boles's images from 2010 Jan. 17 and Mar. 4 (limiting mag 19.5) or onDigitized Sky Survey plates from 1989 Dec. 21 (limiting red mag 20.5) and1990 Jan. 1 (limiting blue mag 21.0).

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars.

P. Challis and R. Kirshner, Harvard-Smithsonian Center for Astrophysics(CfA); and N. Smith, University of Arizona, on behalf of the CfA SupernovaGroup, report that spectroscopic observations (range 320-850 nm) of 2010jr(cf. CBET 2545), obtained on Nov. 14.3 UT with the MMT (+ blue-channelspectrograph), show a smooth and very blue continuum that resembles thatseen in spectra of SN 1993J from two weeks before maximum light. A spectrumof 2010jp (cf. CBET 2544) shows the Balmer series lines of a type-IInsupernova; broad red wings extend to +15000 km/s, with much sharperabsorptions on the blue side at approximately -3000 km/s, which resemble theline profiles seen in spectra of SN 2006gy. A spectrum of 2010js (cf. CBET2546) shows the symmetric Balmer lines with widths of approximately 4000km/s (FWZI) seen in type-IIn supernovae; the redshift for this object in UGC4294 is z = 0.039.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars.

R. Kirshner and P. Challis, Harvard-Smithsonian Center for Astrophysics(CfA); and T. Matheson, National Optical Astronomical Observatory, on behalfof the CfA Supernova Group, report on spectroscopic observations (range320-850 nm) obtained on Nov. 16.3 UT with the MMT (+ blue-channelspectrograph) of the three apparent supernovae announced on CBET 2549.Cross-correlation with a library of supernova spectra using the "SupernovaIdentification" code (SNID; Blondin and Tonry 2007, Ap.J. 666, 1024) indicatesthat 2010ju is a type-Ia supernova about one week before maximum light; thevelocity of the Si II minimum is blueshifted by about 16000 km/s in thesupernova's restframe. The spectrogram of 2010jv shows the spectrum of atype-Ia supernova at maximum, with a blueshift of 11000 km/s at the Si IIline. The spectrogram of 2010jw has a spectrum that resembles the type-Icsupernova 2004eu at five days past maximum light.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars.

It is with deep regret that we must announce the death todayof Brian G. Marsden after a lengthy illness. He will be rememberedas contributing much to celestial mechanics and the dynamics andorbits of minor bodies of the solar system and as having an encyclopedicknowledge of the history of astronomy. He was a dedicated servant tothe astronomical community for many decades, serving as Director of theCentral Bureau from 1968 to 2000 (and as Director Emeritus since then)and as Director of the Minor Planet Center from 1978 to 2006 (and asDirector Emeritus since then). He also served extensively withinCommissions 6 and 20 of the IAU over the years, being past President ofboth Commissions. And he was one of the most visible astronomers inthe world over the years in terms of his generous availability to thenews media on behalf of the astronomical community.

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U. Munari and A. Siviero, Istituto Nazionale di Astrofisica, PadovaAstronomical Observatory; R. L. M. Corradi, Instituto de Astrofisica deCanarias; and P. Valisa, G. Cherini, F. Castellani, and S. Dallaporta, "AsiagoNovae and Symbiotic Stars" (ANS) collaboration, report that the symbiotic starAX Per is undergoing a brightening phase, the first after the short outburstit experienced in the (northern-hemisphere) spring of 2009 (cf. CBET 1757).The 2009 event was the first bright phase after the major outburst AX Perexperienced between 1988 and 1992 (cf. IAUCs 4544, 4621, 4922, 4994). Themonitoring carried out with several ANS-collaboration telescopes recorded AXPer to be still in quiescence at B = 12.33 (B-V = +0.89, V-I_c = +2.79) on2010 Nov. 15.93 UT. On Nov. 19.97, it had brightened to B = 11.73 (B-V =+0.80, V-I_c = +2.53), and by Nov. 22.69 it has reached B = 11.63 (B-V =+0.78, V-I_c = +2.47). Interestingly, the start of this new active phase isoccurring about 615 days past that of 2009, which is not too dissimilar fromthe orbital period of the star (682 days). Absolute opticalspectrophotometry of AX Per was obtained with the 0.60-m telescope of theSchiaparelli Observatory in Varese. The spectrum from Nov. 22 ischaracterized by a strong and high-ionization emission-line spectrum,superimposed on the M-giant absorption spectrum, which is veiled shortwardof 500 nm by the blue continuum from circumstellar nebular material. Onthis spectrum, the integrated flux of H_beta emission is 1.2 x 10**(-11)erg cm**(-2) s**(-1), and the flux ratios (H_beta):(H_alpha):(He II468.6-nm):(He I 587.6-nm):([O III] 500.7-nm):([Fe VII] 608.7-nm):(O I844.6-nm) are 1.00:5.18:0.47:0.22:0.19:0.0067:0.069; for comparison, onAugust 7, during quiescence, they obtained exactly the same flux for H_betaemission, but different line ratios 1.00:6.01:0.24:0.24:0.05:0.068:0.16. Sothe onset of the current active phase has not changed the flux of Balmer andHe I lines, but increased He II by a factor of two and [O III] by three,and reduced O I 844.6 by a factor of two and [Fe VII] by ten. It is worthnoting that AX Per underwent a short-duration flare about one year beforethe onset of the major 1988-1992 outburst. It is tempting to speculate bysimilarity that the 2009 short outburst could be a similar precursor, andthat the present rise in brightness by AX Per could be the onset of a majoroutburst event similar to that in 1988-1992.

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J. Vinko, University of Szeged; W. Zheng and A. Romadan, University ofMichigan; R. Quimby, California Institute of Technology; N. Whallon, S. B.Pandey, Y. Fang, and C. Akerlof, University of Michigan; P. Pasque and M.Verkinderen, Cousino High School; and J. C. Wheeler and E. Chatzopoulos,University of Texas, on behalf of the ROTSE collaboration, report the discoveryof a new supernova (mag about 17.5) in unfiltered images taken on Nov. 14.49 UTwith the 0.45-m ROTSE-IIIb telescope at McDonald Observatory. The new object-- which was observed again on Nov. 16.49 at mag about 17.4, on Nov. 18.48 atmag about 17.4, and on Nov. 22.47 at mag about 17.5 -- is located at R.A. =12h08m01s.11, Decl. = +49o13'31".1 (equinox 2000.0; uncertainty about 1"),which is 2".1 east and 1".8 south of the center of the presumed host galaxy(SDSS J120800.89+491332.8). Note that there is a fainter, uncataloguedextended source about 2" southeast of the host galaxy that is also a possiblecandidate to be the host galaxy of the new supernova. A finding chart for thenew object can be found at the following website URL:http://www.rotse.net/rsvp/j120801.1+491 ... 491331.jpg. A spectrum,obtained on Nov. 22.51 UT with the 9.2-m Hobby-Eberly Telescope (+ MarcarioLow-Resolution Spectrograph) by J. Caldwell, shows broad, weak P-Cyg featuressuperimposed on a blue continuum, consistent with an early type-II supernova.If the strongest broad feature is due to H-alpha, then the redshift is z about0.1, implying a peak absolute magnitude brighter than -20.5 (neglectinginterstellar extinction). According to SNID (Blondin and Tonry 2007, Ap.J.666, 1024), the spectrum is similar to that of SN 1999gi at 5 days beforemaximum light at a redshift consistent with the above estimate, but notemplate matches all the observed features well. These suggest that thesupernova may be a peculiar, super-luminous event.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars.

W. Zheng, University of Michigan; J. Vinko, University of Szeged; R.Quimby, California Institute of Technology; A. Romadan, N. Whallon, S. B.Pandey, F. Yuan, and C. Akerlof, University of Michigan; P. Pasque and M.Verkinderen, Cousino High School; and J. C. Wheeler And E. Chatzopoulos,University of Texas, on behalf of the ROTSE collaboration, report thediscovery of a new supernova (mag about 18.1) in unfiltered images taken onNov. 14.34 UT with the 0.45-m ROTSE-IIIb telescope at McDonald Observatory.The new object -- which was observed again on Nov. 23.11 at mag about 18.0and on Nov. 24.06 at mag about 18.2 -- is located at R.A. = 0h57m24s.62,Decl. = -0o57'51".4 (equinox 2000.0; uncertainty about 1"), which is 0".2east and 1".9 south of the center of the presumed host galaxy (SDSSJ005724.60-005749.5). A finding chart for the object can be found atwebsite URL http://www.rotse.net/rsvp/j005724.6-005 ... 005751.jpg.A spectrum, obtained on Nov. 25.10 UT with the 9.2-m Hobby-Eberly Telescope(+ Marcario Low-Resolution Spectrograph) by S. Odewahn, shows 2010ke to be atype-Ia supernova at more than a week after maximum light. The spectrumcontains a strong Si II feature and several other broad lines of S II and FeII, characteristics of type-Ia supernovae. The best-matching templatespectrum in SNID (Blondin and Tonry 2007, ApJ. 666, 1024) is to the spectrumof SN 1995E at 10 days after maximum. The redshift, estimated from broadsupernova features, is z = 0.042, consistent with the photo-z estimate ofthe presumed host galaxy in the SDSS database. The expansion velocity atthe photosphere, derived from the absorption minimum of the Si II 635.5-nmfeature, is about 10000 km/s.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars.